The structure and characteristics of the accretion disk were calculated using our MHD model of the accretion disks [1]}, which is based on the model of [2]}. The vertical structure of the disk at each radial distance \(r\)  is calculated from the solution of the hydrostatic equilibrium equation for the case of polytropic gas. It is considered that the turbulent friction is the main heating mechanism inside the disk. There is optically thin corona above the optically thick disk. The temperature of the corona is determined by the heating of the gas with incident stellar radiation. We adopted that the fraction of the radiation flux intercepted by the disk's surface is constant, \(f=0.05\) , at every \(r\) . Transition from the disk to its corona is treated as hydrostatic region with exponential growth of gas temperature over the local scale height of the disk.
